Cosmic Evolution of Size and Velocity Dispersion for Early Type Galaxies
L. Fan (1,2), A. Lapi (3,1), A. Bressan (4,1), M. Bernardi (5), G. De, Zotti (4,1), and L. Danese(1) (1-SISSA/ISAS, Trieste, Italy, 2-Univ. of Sc., and Tech., China, 3- Univ. `Tor Vergata', Roma, Italy, 4-INAF, Padova, Italy,, 5-Univ. of Pennsylvania, Philadelphia, USA)

TL;DR
This paper investigates the size and velocity dispersion evolution of early type galaxies from high redshift to the present, proposing that quasar activity influences their structural growth over cosmic time.
Contribution
It introduces a model linking quasar activity to the size increase of early type galaxies, explaining observed size evolution and density changes from high redshift to today.
Findings
High-z ETGs are denser within the same physical radius.
Size evolution is mainly significant at z>1.
Quasar activity may cause rapid size increase via gas removal.
Abstract
[abridged] Massive, passively evolving galaxies at redshifts z>1 exhibit on the average physical sizes smaller by factors ~3 than local early type galaxies (ETGs) endowed with the same stellar mass. Small sizes are in fact expected on theoretical grounds, if dissipative collapse occurs. Recent results show that the size evolution at z<1 is limited to less than 40%, while most of the evolution occurs at z>1, where both compact and already extended galaxies are observed and the scatter in size is remarkably larger than locally. The presence at high z of a significant number of ETGs with the same size as their local counterparts as well as of ETGs with quite small size, points to a timescale to reach the new, expanded equilibrium configuration of less than the Hubble time. We demonstrate that the projected mass of compact, high-z galaxies and that of local ETGs within the *same physical…
Peer Reviews
No public reviews on file for this paper yet. If you reviewed it on a platform where reviews are public (OpenReview, ICLR, NeurIPS, ICML), you can paste yours below so the community can read it here.
Videos
No videos yet. Explain this paper in a talk, walkthrough, or lecture? Add one.
